As the bulk of RU Lup's accretion variability cannot be due to stellar rotation nor to extinction, it must then be related to variations of the mass accretion rate (a factor of 2 or 0.31 dex, see Table REF ) onto the star during our 15-day spectroscopic monitoring. On our observational timescale, such variability is similar to what was found in other photometric and spectroscopic studies of CTTSs [1]}, [2]}, [3]}.
